MRI channel flows in vertically stratified models of accretion discs

@article{Latter2010MRICF,
  title={MRI channel flows in vertically stratified models of accretion discs},
  author={Henrik N. Latter and S{\'e}bastien Fromang and O. Gressel},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2010},
  volume={406},
  pages={848-862}
}
Simulations of the magnetorotational instability (MRI) in ‘unstratified’ shearing boxes exhibit powerful coherent flows, whereby the fluid vertically splits into countermoving planar jets or ‘channels’. Channel flows correspond to certain axisymmetric linear MRI modes, and their preponderance follows from the remarkable fact that they are approximate non-linear solutions of the MHD equations in the limit of weak magnetic fields. We show in this paper, analytically and with one-dimensional… Expand
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Jets, from the protostellar to the AGN context, have been extensively studied but their connection to the turbulent dynamics of the underlying accretion disc is poorly understood. Following a similarExpand
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References

SHOWING 1-10 OF 49 REFERENCES
SUSTAINED MAGNETOROTATIONAL TURBULENCE IN LOCAL SIMULATIONS OF STRATIFIED DISKS WITH ZERO NET MAGNETIC FLUX
We examine the effects of density stratification on magnetohydrodynamic turbulence driven by the magnetorotational instability in local simulations that adopt the shearing box approximation. OurExpand
MRI channel flows and their parasites
Local simulations of the magnetorotational instability (MRI) in accretion discs can exhibit recurrent coherent structures called channel flows. The formation and destruction of these structures mayExpand
What is the Numerically Converged Amplitude of Magnetohydrodynamics Turbulence in Stratified Shearing Boxes
We study the properties of the turbulence driven by the magnetorotational instability in a stratified shearing box with outflow boundary conditions and an equation of state determined byExpand
Magnetorotational instability in stratified, weakly ionized accretion discs
We present a linear analysis of the vertical structure and growth of the magnetorotational instability in stratified, weakly ionized accretion discs, such as protostellar and quiescent dwarf novaeExpand
Parasitic instabilities in magnetized, differentially rotating disks
Velikhov, Chandrasekhar, Balbus & Hawley have discovered a MHD instability of differentially rotating fluids that may explain the effective viscosity of accretion disks. If the unperturbed magneticExpand
Angular momentum transport in protostellar discs
Angular momentum transport in protostellar discs can take place either radially, through turbulence induced by the magnetorotational instability (MRI), or vertically, through the torque exerted by aExpand
The Evolution of Channel Flows in MHD Turbulence Driven by Magnetorotational Instability
MHD turbulence driven by magnetorotational instability (MRI) in accretion disks is investigated using the local shearing box calculations. The growth of many short-wavelength MRI modes, which areExpand
Local Magnetohydrodynamic Models of Layered Accretion Disks
Using numerical MHD simulations, we have studied the evolution of the magnetorotational instability (MRI) in stratified accretion disks in which the ionization fraction (and therefore resistivity)Expand
High accretion rates in magnetised Keplerian discs mediated by a Parker instability driven dynamo
Hydromagnetic stresses in accretion discs have been the subject of intense theoretical research over the past one and a half decades. Most of the disc simulations have assumed a small initialExpand
Dynamo-generated Turbulence and Large-Scale Magnetic Fields in a Keplerian Shear Flow
The nonlinear evolution of magnetized Keplerian shear ows is simulated in a local, three-dimensional model, including the eeects of compressibility and stratiication. Supersonic ows are initiallyExpand
...
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2
3
4
5
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